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Astrophysical Jet Around Compact Objects: a Source for HEN and GW ?

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Astrophysical Jet Around Compact Objects: a Source for HEN and GW ? Astrophysical jet around compact objects: A source for HEN and GW ? Fabien CASSE Laboratoire AstroParticule & Cosmologie (APC) Université Paris Diderot Active Galactic Nuclei • The core of the AGN is a black hole surrounded by an accretion disk. • Various classes of AGN with different characteristics (FR 1 and FR 2). • FR2 AGN are the most powerful high- energy emitters among AGN. • Low emitting jets ending into bright, extended “hotspots”. • “Blazars” seems to be interesting objects for the production of HE astroparticles (TeV emission). • Search for HE neutrinos is linked to the search of UHECR sources. • Recent Auger results suggest that UHE (1995) cosmic rays come from AGN (real source or last scattering centers for CR from GRBs? See e.g. Kotera & Lemoine Padovani 2008). & Urry Urry Blazars • Blazars are believed to be FR2 jets aligned with our line of sight. • Powerful emission ranging from VLBI up to TeV γ-rays. • The variability of the source shows that the emitting region has a size of ≤ 1013cm. • The emitting region is a small region containing relativistic particles --> Relativistic beaming enhances the radiative emission. • The first hump feature is believed to arise from synchrotron emission by relativistic electrons --> presence of significant magnetic field. • The nature of the second hump is still a matter of debate.. •Leptonic models: the second hump produced by SSC emission of a relativistic pair plasma. •Hadronic models: the HE bump is created by proton induced cascades (pp collision or pγ photo-desintegration via Δ-resonance). Microquasars • Binary compact objects (BH or NS) surrounded by an accretion disk. • Compact objects likely to be stellar black hole (M ~3-10 M). • Binary systems located in our close environnement (d~ few kpc). • Angular resolution is quite poor compared to AGN ! • Mildly relativistic large-scale jet which velocity ranges from Vjet~0.1 to 0.95c. • Multi-wavelength (Radio to X-ray) emission from both the disk and jets. • Composition of the jet is still an issue (except for SS433 -> baryonic). • Quasi-Periodic Oscillations (QPO) in X-rays emission question the accretion process. Chaty et al. (1998) Compact objects & Jets • What is the energy source able to power the jets ? – Rotation energy of a spinning black hole: – Energy released by accretion of mass: • Accretion is the most likely reservoir of energy. • Still need to have an extra mechanism to give birth to relativistic particles able to radiate non-thermal emission.. • What about cosmic ray acceleration ? 21 – AGN: Emax ~ 10 eV 17 – Microquasars: Emax ~10 eV Accretion disks & Jets • Jets can be launched from accretion disks thank to a MHD energy transfer (Blandford & Payne 1982). • Collimation is ensured by the pinching effect of the toroidal magnetic field. • Jets launched by disks cannot reach relativistic bulk velocities ! • Hollow structure enables additional non-thermal particle acceleration to take place along the jet axis. Casse & Keppens (2004) Leptonic models o These models are based on the birth of a dense, relativistic pair plasma in a strongly magnetized region. o The pair plasma is either produced by: – Interaction of the rotating massive black hole with a surrounding magnetic field (Blandford-Znajek 1977) -> works only if the accretion disk is underluminous.. – The comptonization of the accretion disk photons (up to UV/X rays) with external jet electrons (e.g. Henri & Pelletier 1991). o The acceleration of the pair plasma is sustained by interaction with MHD wave turbulence from external jet (Γ ~10). o Small fraction of protons seems able to be accelerated by the e+-e- pairs. No significant neutrino emission expected !! Hadronic models o The sub-pc relativistic jet is made of proton-electron plasma. o The relativistic electrons produce the low energy synchrotron emission. o The collisions of relativistic protons with ambient matter and photon field generate secondary particles o High energy γ-rays and neutrinos will be produced altogether ! o Several types of model: 9 -3 o Pp collisions: require very large ambient plasma density (np > 10 cm ) - -> leads to (too) large total energy in AGN jets but may be alright in microquasar jets.. o Photohadronic model: take into account either the internal synchrotron emission or the photon field produced by the accretion disk or both of them ! Neutrinos emission from jets • Various authors have addressed the issue of UHE neutrino production doing different assumptions: • Heavy jets (high density protons) leading to dominant p+p collisions (e.g. Atoyan & Dermer, Schuster et al.,Heinz, Romero et al., etc..) --> the surrounding plasma density has to be large which is quite challenging for the jet launching in AGN.. • Relativistic jet encountering a dense photon field (Stecker et al., Levinson & Waxman, Mannheim et al., Bednarek & Protheroe, Aharonian et al.,etc…). • Both AGN and microquasars jets are believed to be optically thin to cosmic ray production, thus prone to the Waxman-Bahcall limit. 2 -8 2 • Studies generally provides upper neutrinos flux around E Φν ~ 10 GeV/ cm s sr which may be detectable by km3 neutrino observatories --> stretching the parameters of the acceleration model and/or physical environnement .. • Recent study have highlighted the impact of the jet strong magnetic field upon neutrino production attenuation (Reynoso & Romero 2009) --> Synchrotron cooling may affect π+- and thus lead to strong attenuation of neutrino spectrum beyond 10 TeV in microquasars. What about AGN hotspots ? • AGN jet hotspots are quite large (L>1kpc), magnetized (B>0.1 mG) region emitting strong X- ray radiations in the vicinity of a shock. • Computations linking MHD simulations to Fokker-Planck calculations provide cosmic ray and electron spectra with secondary particles produce by pp and pγ collisions. • Some hotspots (e.g. 3C273A) are able to accelerate particle up to 1020 eV. • Neutrinos (up to 1018 eV) can be produce altogether with γ-rays. • Nevertheless, hotspots are very diluted -7 -3 (np~2x10 cm ) and remote objects (> 50 Mpc) leading to a very weak neutrino flux 2 -15 2 --> E Φν ~ 10 GeV/ cm s Casse & Marcowith (2005) GW and microquasars • Sudden accretion onto a black hole or a neutron star can lead to GW whose amplitude is 1/ 2 1/ 2 "1 % #m ( % f (" % d ( h ~ 10"20' * ' * Price (1972) "6 ' * Nagar et al.(2007) & 10 M$ ) & 1kHz) & 1kpc ) • Such signal would be associated with extremely ! powerful outburst from the accretion disk (PACC ~ 1047 erg/s!!). • Ejection of mass from a black hole can also generate GW whose amplitude is $ ' "22$ # ' *m h ~ 10 & )& "6 ) Segalis & Ori (2001) % 10(% 10 M+ ( • Ejection must come from the black hole itself, Pradier (2008) which seems doubtful… ! Summary • Detection of HE neutrinos coming from AGN and/or microquasars would have a tremendous impact on models dealing with the physics of ejection (nature of the relativistic flow, constraints on acceleration, magnetic field, etc…). • It would also be a “smoking gun” for cosmic ray acceleration within these structures. • The variability of the HE neutrino emission would also help to characterize the accretion process occurring near black hole (especially in microquasars where variability scales over short periods). • Non-detection of HE neutrinos coming from AGN and/or microquasars would not be conclusive as it might be either because relativistic jets are leptonic or because the neutrino flux is too weak. • GW detection from microquasars would be a huge surprise since it would imply accretion parameters far beyond what is expected -->It would also imply finding brand new ideas to explain the related catastrophic accretion onto black hole..
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